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SWI_2D_MAP_OTF_CCH_V1Similar to SWI 2D MAP PS, but using an on-the-fly recording sequence, i.e. the OFF position per map row is only observed once.SWI
SWI_2D_MAP_OTF_V1Similar to SWI 2D MAP PS, but using an on-the-fly recording sequence, i.e. the OFF position per map row is only observed once.SWI
SWI_NADIR_STARE_FS_V1Same as SWI NADIR STARE PS, except a frequency-switch calibration mode is used instead of position-switch. It enables spending  100% of the integration time on-source. If the purity of the spectral band is good enough, there is an option to pre-compute ON-OFF for the CTS before downlink.SWI
SWI_NADIR_STARE_PS_V1Investigation of the atmospheric composition (and temperature) of Jupiter and the Galilean moons. This mode is nominally meant for deep integrations and requires numerous repetitions (e.g. monitoring of the moons). Two CTS spectra are recorded for 60 seconds over 10000 channels (16 bits coding). Position-switch calibration method.SWI
SWI_TSYS_ACS_CCH_V1Spectral scan to measure the system temperature spectra of the 2 bands with the ACS & CCH 1 & 2 by observing the hot load and cold sky. Integration time on ACS is 1 second. A single execution can cover up to 15 tunings.SWI
UVS_SAT_LIMB_SCAN_HPSimilar to disc scan observations, but holding the pointing relative to the limb during flyby sequences.UVS
UVS_SAT_LIMB_SCAN_APSimilar to disc scan observations, but holding the pointing relative to the limb during flyby sequences.UVS
UVS_SAT_LIMB_STARE_HPSearch for faint atmospheric emissions by building signal to noise through long integrations.UVS
UVS_SAT_LIMB_STARE_APSearch for faint atmospheric emissions by building signal to noise through long integrations.UVS
UVS_SAT_DISK_SCAN_HPConstruct spectral image cubes of multiple atmospheric emission line features (up to 1024 selectable spectral bins with a minimum of 3 key emissions: H Lya, OI 130.4 nm, OI 135.6 nm), with repeated scans to investigate highly time-variable auroral dynamics.UVS
UVS_SAT_DISK_SCAN_APConstruct spectral image cubes of multiple atmospheric emission line features (up to 1024 selectable spectral bins with a minimum of 3 key emissions: H Lya, OI 130.4 nm, OI 135.6 nm), with repeated scans to investigate highly time-variable auroral dynamics.UVS
UVS_NC_STARECharacterize the Io/Europa neutral clouds in the immediate vicinity of the satellite. Center satellite in slit. Align the slit with the satellite orbital planeUVS
UVS_IO_TORUS_STAREMonitor emissions from the Io torus. Slit aligned parallel with Jupiter's equator.UVS
UVS_GCO_HISTOGRAM_003Similar to observation 001 but with increased spectral resolution to achieve < 2 nm resolution between 100 and 200 nm as specified in SciRDUVS
DRAFT_3GM_BSRCharacterisation of the surface by determination of roughness, dielectric constant of surface material and material density. The chosen antenna points towards surface, radio signal reflects from surface and received on ground. USO unmuted. The HAA shall be ON to calibrate the sloshing potentially excited by pointing the HGA toward a moon’s Surface.3GM
DRAFT_3GM_OCCULTATIONThe radio science experiment 3GM, with its dual-frequency radio links (X and Ka-band) referenced to an ultrastable oscillator (USO), is performed as JUICE spacecraft moves in and out of occultation. Occultations occur throughout the jovian tour, but their phasing is not always synchronized with the timing of dedicated Jupiter observations by the other orbiter experiments. USO unmuted, HAA in NOMINAL SCIENCE. Note that 2 other options exist for torus occultations but are not (yet) defined in the database3GM
DRAFT_3GM_GRAVITY_TOURKaT and HAA should be operating during gravity measurement USO assumed to be ON during the full tour: this should be defined in the scenario set-up and not at 3GM observation approach. HAA should be in STANDBY mode at least 48 hours before the gravity measurement. The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up.3GM
DRAFT_3GM_GRAVITY_GCO500_200Gravity measurement during GCO500 and GCO200 will use the HGA during downlink sessions. If not possible, it will use the MGA. KaT and HAA should be operating during gravity measurement. USOis OFF during this phase (except in case of BSR opportunity). HAA should be in STANDBY mode at least 48 hours before the gravity measurement. The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up.3GM
DRAFT_3GM_GRAVITY_FLYBYSGravity measurement during flyby requires the use of the MGA. KaT and HAA should be operating during gravity measurement USO assumed to be ON during the full tour: this should be defined in the scenario set-up and not at 3GM observation approach. HAA should be in STANDBY mode at least 48 hours before the gravity measurement. The observation should start with 1 hour of HAA in CALIBRATION mode. KaT starts with 10min of warm-up.3GM
UVS_JUP_ROLL_SCANPoint to nadir. Rotate about nadir so that we scan a circle (or a fraction of a circle - e.g. covering the auroral regions) over Jupiter's disk. Rotation rate ~0.1 degree per secondUVS
GAL_GAN_OFF_POINTINGspecific observation for polar geometry with off-pointing w.r.t Nadir during GCO500. Only to be executed TBD time. Similar profile than GAL_MONITORING_GAN but with off nadir pointing requestGALA
GAL_WARMUP_GANneeded right before ANY science observation from GALA during Ganymede phase Duration: 90minGALA
JAN_SCI_INERTIALTBWJANUS
JAN_SCI_LIMB JANUS
PEP_GANYMEDE_IN_SITU_LOW_8Only PEP-Hi on (all in-situ), max power savings PEPLo Sensors ON: None PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_LOW_7Mode with only NIM on (ion) from PEP-Lo. Required for avoiding switching on/off NIM once per day during downlinks. Good for long surveys of the ionosphere. PEP Hi on, all in-situ PEPLo Sensors ON: NIM ion on, only PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_LOW_6Mode with only NIM on (neutral) from PEP-Lo. Required for avoiding switching on/off NIM once per day during downlinks. Good for long surveys of the exosphere. PEP Hi on, all in-situ. PEPLo Sensors ON: NIM neutral on, only PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_NOMINAL_3Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey in charged particles. NIM, JNA off. PEP Hi on, all in-situ. PEPLo Sensors ON: JDC, JEI on, JNA & NIM off PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_NOMINAL_2Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey. All instruments on, NIM in ion mode (response of ionosphere to charged particles). PEP Hi on, all in-situ PEPLo Sensors ON: All sensors ON, NIM, JNA ion mode PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_NOMINAL_1Regular in-situ mode, ganymede phase. CA of moon flybys later in the mission (higher power consumption). Good for high quality, extended survey. All instruments on, NIM in neutral mode (response of exosphere to charged particles). PEP Hi on, all in-situ PEPLo Sensors ON: All sensors ON, NIM neutral mode, JNA ion mode PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_BURST_1Burst in-situ mode, Ganymede phase. CA of moon flybys later in the mission (higher power consumption) Short duration events (e.g. boundary crossings). All instruments on, NIM in neutral mode (response of ionosphere to charged particles). PEP Hi on, all in-situ PEPLo Sensors ON: All sensors ON, NIM neutral mode, JNA ion mode PEPHi Sensors ON: JENI_Ion, JoEEPEP
RIM_GANYMEDE_O1_1Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km considering on-board processing with presuming factor Np of 1.RIME
RIM_GANYMEDE_O1_2Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km considering on-board processing with presuming factor Np of 2.RIME
RIM_GANYMEDE_O1_4Ganymede Optional Acquisitions (O1) in low vertical resolution (LR) mode at high penetration depth until 15km processing with presuming factor Np of 4.RIME
RIM_GANYMEDE_N4Passive Radar Acquisitions on Jovian side of Ganymede.RIME
RIM_GANYMEDE_N3_1Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 1.RIME
RIM_GANYMEDE_N3_2Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 2.RIME
RIM_GANYMEDE_N3_4Ganymede Nominal Acquisitions (N3) in high vertical resolution (HR) mode until 4km depth in the anti-Jovian side of Ganymede in order to complete the SRM on high-interest targets considering on-board processing with presuming factor Np of 4.RIME
RIM_GANYMEDE_N2_1Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 1.RIME
RIM_GANYMEDE_N2_2Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 2.RIME
RIM_GANYMEDE_N2_4Ganymede Nominal Acquisitions (N2): in low vertical resolution (LR) mode until 9km depth in the Jovian side of Ganymede considering on-board processing with presuming factor Np of 4.RIME
RIM_GANYMEDE_N1_1Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 1.RIME
RIM_GANYMEDE_N1_2Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 2.RIME
RIM_GANYMEDE_N1_4Ganymede Nominal Acquisitions (N1) in low vertical resolution (LR) mode until 9km depth in the anti-Jovian side of Ganymede considering on-board processing with presuming factor Np of 4.RIME
RIM_GANYMEDE_FLYBYRIME flyby observations or observations without on-board processing.RIME
NAVCAM_DVOL_BLOCK JUICE
MAG_DL_FOB_LIGHT_ONLYThis observation is introduced to characterise JMAG operations during downlink times where power resources from the SC may be more limited, and where SC attitude is driven by operational constraints In this particular observation FOB fluxgate is powered on with FSC as light-only.JMAG
MAG_DL_LIGHT_ONLYThis observation is introduced to characterise JMAG operations during downlink times where power resources from the SC may be more limited, and where SC attitude is driven by operational constraints. In this particular observation FIB & FOB fluxgates powered on with FSC as light-only.JMAG
PEP_GANYMEDE_IN_SITU_LOW_2Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JE 4 sectors, JDC low power). NIM neutral, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments. PEP Hi on, all in-situ. PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Neutral mode PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_LOW_5Same as PEP_GANYMEDE_IN_SITU_LOW_1 but with lowest performance in JDC, JEI for max power savings while PEP-Lo is no (JEI 4 sectors, JDC low power). NIM, JNA off. Low power mode for Ganymede, good for long duration surveys. PEP Hi on, all in-situ PEPLo Sensors ON: JDC_LP, JEI 4 sectors, JNA & NIM off PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_JUPITER_IN_SITU_LOW_1Low power in-situ mode (e.g. downlink, non-prime/low priority science sgments) PEPLo Sensors ON: JDC_LP, JEI (8 sectors) PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_JUPITER_IN_SITU_BURST_1Burst in-situ mode for magnetosphere, CA of moon flybys (if NIM offl), Short duration events (magnetopause/bow shock crossings, injection events, moon wakes/microsignatures) PEPLo Sensors ON: JDC, JEI PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_LOW_3Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JEI 4 sectors, JDC low power). NIM ion, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments. PEP Hi on, all in-situ PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Ion mode PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_LOW_4Same as PEP_GANYMEDE_IN_SITU_NOMINAL_1 but with low performance in JDC, JEI to limit power (JEI 4 sectors, JDC low power). NIM ion, JNA on. Low power mode for Ganymede, good for long duration surveys with multiple instruments. PEP Hi on, all in-situ PEPLo Sensors ON: JEI: 4 sectors, JDC: LP, NIM: Ion mode PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_BURST_2Burst in-situ mode, Ganymede phase. CA of moon flybys later in the mission (higher power consumption) Short duration events (e.g. boundary crossings). All instruments on, NIM in neutral mode (response of ionosphere to charged particles). PEP Hi on, all in-situ PEPLo Sensors ON: All sensors ON, NIM, JNA ion mode PEPHi Sensors ON: JENI_Ion, JoEEPEP
PEP_GANYMEDE_IN_SITU_LOW_1Same as PEP_GANYMEDE_IN_SITU_NOMINAL_3 but with low performance in JDC, JEI to limit power (JEI 8 sectors, JDC low power). NIM, JNA off. Low power mode for Ganymede, good for long duration surveys PEP Hi on, all in-situ PEPLo Sensors ON: JDC_LP, JEI (8 sectors) PEPHi Sensors ON: JENI_Ion, JoEEPEP
MAG_CONTINOP_FIB_FOB_LIGHT_ONLYJMAG mode (FIB FOB Light Only), this mode ensures that while FIB and FOB are collecting science the Scalar sensor also has power to its laser but is not collecting science data. This helps to protect the fibres from radiation damage, necessary for the Europa phase due to its radiation environment.JMAG
SWI_SCIENCEPlace holder: one of the ASW mode, where the science script will be run ( i.e. from SWI_TSYS_CTS down to SWI_MOON_NADIR_STARE_FS) during the missionSWI
SWI_SPECTRAL_SCAN_CTS_FS_V1Same as SWI SPECTRAL SCAN CTS PS, except a frequency-switch calibration mode is used instead of position-switch. It enables spending  100% of the integration time on-source. If the purity of the spectral band is good enough, there is an option to precompute ON-OFF for the CTS before downlink. A single execution can cover up to 9 tunings.SWI
SWI_SPECTRAL_SCAN_CTS_PS_V1Investigation of the atmospheric composition of Jupiter and the Galilean moons. The whole frequency range available to SWI is scanned. This mode is nominally meant for deep integrations and requires numerous repetitions (e.g. monitoring of the moons). Two CTS spectra are recorded for 60 seconds over 10000 channels (16bit coding). Position-switch calibration method. A single execution can cover up to 13 tunings. Pointing Type: S/C: nadir or limb. Instrument: nadir or limb, using the SWI mechanism if S/C points nadir and to reach the moonsSWI
SWI_SPECTRAL_SCAN_ACS_FS_V1Same as SWI SPECTRAL SCAN ACS PS, except a frequency-switch calibration mode is used instead of position-switch. It enables spending  100% of the integration time on-source. The ACS does not allow to pre-compute ON/OFF before downlink. A single execution can cover up to 11 tunings.SWI
SWI_SPECTRAL_SCAN_ACS_PS_V1Investigation of the atmospheric composition of Jupiter and the Galilean moons. The whole frequency range available to SWI is scanned. This mode is nominally meant for deep integrations and requires numerous repetitions (e.g. monitoring of the moons). Two ACS spectra are recorded for 60 seconds over 1024 channels. Position-switch calibration method. A single execution can cover up to 16 tunings.SWI
PEP_FLYBY_FAR_DEPARTURE_LOW_RATE_ENAEuropa environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations) Europa imaging (JNA) & Europa torus (JNA imaging + in-situ) All sensors on except NIM (in standby or off). JENI in Combo mode (half in ion mode, half imaging) NIM in ram direction (X-Y S/C plane)PEP
PEP_FLYBY_FAR_DEPARTURE_LOW_RATEEuropa environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations) Europa imaging (JNA) & Europa torus (JNA imaging + in-situ) All sensors on except NIM (in standby or off). Corotation in JEI or JDC FoV Full pitch angle coverage (JDC, JEI, JoEE, JENI)PEP
PEP_FLYBY_FAR_DEPARTURE PEP
PEP_FLYBY_DEPARTUREEuropa environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations) Europa imaging (JNA) & Europa torus (JNA imaging + in-situ) All sensors on except NIM (in standby or off) Corotation in JEI or JDC FoV Full pitch angle coverage (JDC, JEI, JoEE, JENI)PEP
PEP_FLYBY_CLOSEST_APPROACHLocal moon-magnetosphere interaction observation: plasma moments, energetic particle spectra and pitch angle distributions (high time resolution for short term variations) Europa imaging (JNA). Dense exosphere (NIM) Sensors on: all Corotation in JEI or JDC FoV Full pitch angle coverage (JDC, JEI, JoEE, JENI) Moon in JNA FoV Angle of NIM_NEUION_S0 from JUICE_EUROPA_RAM or JUICE_GANYMEDE_RAM or JUICE_CALLISTO_RAM velocity less than 5 deg at CA Solar panel rotation angle (SADM) SADM > 74° or SADM < -74° Moon in JNA FoVPEP
PEP_FLYBY_APPROACHMoon environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (low time resolution). Moon imaging (JNA) & Europa torus (JNA imaging + in-situ) if near Europa. High altitude exosphere (NIM) Sensors on: all Corotation in JEI or JDC FoV Full pitch angle coverage (JDC, JEI, JoEE, JENI ions) Moon in JNA FoV Angle of NIM_THERMAL_1 or THERMAL_2 from JUICE_EUROPA_RAM or JUICE_GANYMEDE_RAM or JUICE_CALLISTO_RAM velocity less than 60 degPEP
PEP_FLYBY_FAR_APPROACH_MEDIUM_RATEMoon environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (low time resolution). Europa torus (JNA imaging + in-situ) if near Europa Sensors on: all Corotation in JEI or JDC FoV Full pitch angle coverage (JDC, JEI, JoEE, JENI ions) Moon in JNA FoV Angle of NIM_THERMAL_1 or THERMAL_2 from JUICE_EUROPA_RAM or JUICE_GANYMEDE_RAM or JUICE_CALLISTO_RAM velocity less than 60 degPEP
PEP_FLYBY_FAR_APPROACH_LOW_RATEMoon environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (low time resolution). Europa torus (JNA imaging + in-situ) if near Europa Sensors on: all Corotation in JEI or JDC FoV Full pitch angle coverage (JDC, JEI, JoEE, JENI ions)PEP
PEP_FLYBY_FAR_APPROACH_NIM_BACKGROUNDNIM background measurements part of switch on procedure. Moon environment monitoring: plasma moments, energetic particle spectra and pitch angle distributions (low time resolution). Europa torus (JNA imaging + in-situ) if near Europa Sensors on: all Corotation in JEI or JDC FoV Full pitch angle coverage (JDC, JEI, JoEE, JENI ions)PEP
RIM_EUROPA_FLYBYRIME flyby observations or observations without on-board processingRIME
UVS_IRR_SATObtain reflectance spectra of irregular satellitesUVS
UVS_IO_SCANSimilar to UVS_DISK_SCAN, but including extra emission lines e.g. from S and Cl. Also requires different spatial binning since Io is more distantUVS
UVS_SAT_TRANSITMeasure absorption of Jupiter airglow by satellite atmospheres as they transit Jupiter's disk, to constrain satellite atmospheric composition and variability. Pointing: nadir (Point slit N-S on Jupiter's disk and wait for moon to transit)UVS
UVS_EUR_SCAN_HIGH_RES_OBSOLETESimilar to UVS_DISK_SCAN but higher resolution. pointing: start at -1.5 satellite radii from the satellite centre, scan in the direction perpendicular to the slit across the disk, ending at +1.5 satellite radii from the centreUVS
UVS_SAT_SURF_HPAs UVS_SAT_SURF_AP but using the high resolution port for improved spatial resolution in key surface regionsUVS
UVS_SAT_SURF_APPushbroom observations near flyby closest approach to investigate surface compositionUVS
MAJ_STANDBYAfter switch-on of MAJIS, the Boot SW automatically starts, and performs the primary boot from the PROM (Init fugitive BSW mode). After processor modules initialization, the Boot software goes to STANDBY mode. By default, the ASW Image0 (stored in MRAM0 = ASM0) is autonomously loaded after a timeout of 30 seconds. MAJIS then enters into ASW init Mode and then into SAFE mode. In STANDBY Mode, all channels are off, and only DPU HK SID1 are received. MAJIS needs to be maintained in STANDBY mode using the TC(17,1) in the following cases : - upload (using service 6) of new ASW images (or CUSW, or firmware) into MRAM: FCP-MAJ-070 describes the maintenance process. - upload a new BROWSE Table FCP-MAJ-060 into MRAM - select ASW Image1 and then start ASW Image 1 instead of teh default ASW Image0. FCP-MAJ-062 - any other update of MRAM using service 6MAJIS
MAJ_SERVICEMAJIS in service MODE (1 or 2 channels with FPE/FPA off + AUX w/o loads) SERVICE Mode as soon as one or two channels are switched ON (PE and AUX) From SERVICE, it is possible to return to SAFE mode or to change the status of MAJIS to DIAG2, DIAG3 or SCIENCE Duration: less than 10minMAJIS
MAJ_SAT_LIMB_TRACKContinuous stare observation of a satellite limb during flyby using inertial pointing from satellite, dayside or nightside. Additional offsets within limb by means of internal pointing mirror. Scanning with MAJIS internal mirror. (--> ‘track limb’). Pointing: S/C limb tracking (‘track limb’) satellite otientation: SLIT tangent to the limb (slit not aligned with S/C motion) Duration: 60minMAJIS
MAJ_SAT_LIMB_SCANFlyby observations of the satellite dayside or nightside limbs with vertical (N-S) slews across track, during yaw-steering phase. Satellite offsets to limb around Y-axis (E-W) before each observation, then satellite offsets around X axis (N-S) between each slit acquisition or continuous slew pointing. Pointing: S/C slew scan centred a limb ( ‘Limb slew scan mode’). Satelliteo orientation: Slit tangent to the limb Duration: 60minMAJIS
MAJ_SAT_DISK_SLEWFlyby observations of the satellite surface with vertical (N-S) slews across track, during yaw-steering phase. One or two slews (pole to pole) necessary to complete dayside coverage. Satellite offset around Y-axis (E-W) before each observation, then satellite offsets around X axis (N-S) between each slit acquisition. Pointing: NADIR Pointing, YS, S/C scan (slew) with offset around Y (‘mosaic mode’ tbc). MAJIS slit perpendicular to the ground-track. Satellite orientation: MAJIS slit perpendicular to the ground-track Duration: 30 minMAJIS
MAJ_SAT_DISK_SCANObservation of a distant satellite dayside or nightside surface. Satellite offset required for pointing then disk coverage is achieved using the internal pointing mirror scanning in the Y (N-S) direction. Pointing: NADIR-P with possible offset around Y, YS, MAJIS scan (‘Nadir scan’). Satellite orientation: MAJIS slit perpendicular to the ground-track Duration: 30minMAJIS
MAJ_SAFEInitiated after ASW loading All channels are off and no PE HK are generated. Only ME HK are generated (only DPU ON) From SAFE it is possible 1) to switch OFF MAJIS, 2) to change the status of MAJIS to DIAG1 or SERVICE mode Duration: less than 5minMAJIS
MAJ_Ring_OccultationObservation of a star occulted by the rings Scan windowing of 9 lines centered on the star (1 scan step = 1/3 MAJIS IFOV) possible Pointing: Inertial. For each occultation, transit of TBD min Satellite orientation: Inertial pointing of the S/C towards the position of the star to maintain MAJIS slit fixed on it. These occultation observations need to be consolidated in the future (star atlas, signal, Tint, S/C inertial capabilities). Scan mirror can be used to mitigate APE driftMAJIS
MAJ_MainRING _PhaseCurveObservations of the main rings at various phase angles (N angles), one ansae (always the same), 20 vertical lines Pointing: S/C pointing ring plane at 1.8 R_J (extremity of main rings) Satellite orientation: OFF-NADIR, Ring plane while maintaining horizontal orientation of MAJIS slit, MAJIS scan mode activated for vertical sampling centered on the rings (20 lines) Duration: 200 sec for one observations at a given phase angleMAJIS
MAJ_MainRING _LowPhaseObservations of the main rings (2 ansa), no tracking of azimuthal structure, 20 vertical lines pointing: OFF-NADIR, S/C pointing centered on the extremity of main rings, S/C depointing required for the two ansa Satellite orientation: Maintaining the MAJIS slit parallel to radial axis of main rings, MAJIS scan mode activated for vertical sampling centered on the rings (20 vertical lines) Duration:400 sec (excluding the S/C repointing to the other ansae)MAJIS
MAJ_MainRING _HighPhaseObservations of the main rings (2 ansa) at high phase (forward scattering light), no tracking of azimuthal structure, no spatial binning to increase spatial resolution. Pointing: OFF-NADIR, S/C pointing centered on the extremity of main rings, S/C depointing required for the two ansa Satellite orientation: Maintaining the MAJIS slit parallel to radial axis of main rings, MAJIS scan mode activated for vertical sampling (20 vertical lines) centered on the rings Duration: 400 sec (excluding the S/C repointing to the other ansae)MAJIS
MAJ_JUP_STELLAR_OCCMAJIS will acquire several “subcubes” (number depends upon planet's speed over the sky) around the (fixed) star position, at different angular distances between the star and the planet's limb during the ingress/egress. Each sub-cube spans over several lines (around 6, less if S/C capability allows it) to compensate for possible pointing inaccuracies. Bright far moons can be used instead of stars as sources to decrease the repetition integration (and therefore spatial sampling) as the orbital velocity ranges from ~ 5 km/s at apojove to ~ 13 km/s at perijove satellite orientation: LIMB TANGENT (preferred, otherwise VERTICAL), to minimize straylight duration: About 10min 66 sec (max) for each subcube. Time interval between sub-cubes as small as possible for better vertical coverage. Total number of cubes depends upon relative angular speed between star and limb.MAJIS
MAJ_JUP_LIMB_SLEWThe scan the atmosphere of Jupiter over the limb up to 3000k is performed with a specific slew of the S/C Individual lines are largely overlapped to provide actual supersampling (x 10) in the spatial domain and allow sub-pixel resolution by deconvolution. Typically, we have cubes of about 300 lines by 50 pixels (~7500 km) Pointing type: OFF-NADIR (nominal pointing position over the Jupiter limb), continuous tracking (‘track tangent limb’) satellite orientation:LIMB TANGENT (MAJIS slit tangent to the limb), very slow s/c slew to get oversampling (10 lines corresponding to one pixel IFOV) Duration: 55 min for each cube (300 lines)MAJIS
MAJ_JUP_LIMB_SCANThe MAJIS pointing mirror is used to scan the atmosphere of Jupiter over the limb up to 1500km. Exposure times are optimized for weak limb emissions. The scan mirror step of 1/10 MAJIS IFOV shall constrain the spatial sampling provides a spatial supersampling adequate to reconstruct, by deconvolution, the signal vertical profile at sub-pixel scale. Observations consists in sets of max. 8 cubes at different latitudes, around the limb of the planet. Duration: Typically 20 min for each cube (110 lines), assuming 11 s per lineMAJIS
MAJ_JUP_HIGH_FREQ_MONITORINGThe observing type is designed to study the evolution of atmospheric features at high temporal frequency as well as to map specific atmospheric features at regional scale. Scanning of features on the Jovian disc, on dayside as well as on nightside, with limited latitudinal coverage. MAJIS will acquire one or more several “subcubes” with a limited number of lines (about between 64 and 160) Duration: between 84 and 315 s for each cube, assuming 2.1 s per lineMAJIS
MAJ_JUP_EVENT_MONITORINGStudy of the evolution of unusual phenomena in Jupiter atmosphere, especially in their zonal evolution MAJIS will acquire several “subcubes” with limited number of lines (about 80) as follows: 1. a series of sub-cubes (from 1 to 4) is acquired with the scan mirror to get the coverage of a limited latitude region at all longitudes on the visible side of the planet. Satellite is re-pointed before acquiring each sub-cube 2. the series at previous point is repeated at fixed time intervals (in the order of 1 h, TBC) to monitor the temporal evolution. Pointing type: YS, Series of OFF-NADIR pointings (‘off-nadir scan mode’) satellite orientation: HORIZONTAL Duration: 160 sec for each sub-cube. Time between series defines actual temporal sampling and is variable (zero data rate here). Total duration about 5 h (1/2 of rotation period)MAJIS
MAJ_JUP_DISK_SLEWObservations of Jupiter clouds and spectroscopy of minor gases. Scanning the instrument slit over Jovian disk (vertical direction) by means of the S/C slew. aims to cover the entire equatorial region (-30°:+30°) Pointing: OFF_NADIR, CONTINUOUS SLEW (« continuous S/C scan ») Satellite orientation: HORIZONTAL Duration: 20 min per cubeMAJIS
MAJ_JUP_DISK_SCANObservations of Jupiter clouds and spectroscopy of minor gases. Scanning the instrument slit over Jovian disk (vertical direction) by means of internal pointing mirror, both dayside and nightside. Aims to cover at least the entire equatorial region (-30°:+30°) during low inclination phases and the polar regions during high inclination phase. Duration: typically 20min/cube, max 30 min/cube, assuming 2.1 s per lineMAJIS
MAJ_JUP_DISK_MOSAICA series of several MAJIS_JUP_DISK_SCAN or MAJIS_JUP_DISK_SLEW Spacecraft has to be re-pointed between individual acquisitions. POinting type: YS, NADIR with offset around Y (‘ nadir offset MAJIS scan’’) satellite orientation: HORIZONTAL (preferred) Duration: 3 x (scan-duration + turnaround Y duration). Scan duration from 20 to 40 min depending on the distance from Jupiter. Turnaround ~50 minMAJIS
MAJ_JUP_AURORAL_MAPPINGObservations of Jupiter aurorae. Scanning of the instrument slit over Jovian polar regions, from polar limb to approx. 50°N/S latitudes, with exposure times optimized for weak auroral emissions. Duration: typically, 40 min (200 lines <-> typical size of latitudes where polar ovals are observed)MAJIS
MAJ_JovianRING_MOSAICMosaicking the 2 ring ansa from 90000 to 230000 km. 3 overlapping cubes of 20 vertical lines performed by the scanner (or S/Cslew if compatible with JANUS). This requires re-pointing between individual cubes. Pointing: OFF-NADIR, S/C pointing projected ring plane, S/C depointing required for the two ansa Satellite orientation: Maintaining the horizontal orientation of MAJIS slit, MAJIS scan mode activated for vertical sampling (20 vertical lines) centered on the rings, S/C depointing required for mosaicking each ansa (3 overlapping cubes to perform a radial mosaic of one ansa of the rings with radial distance from 90000 to 230000 km) Duration: 1200 sec (excluding the S/C repointings)MAJIS
MAJ_ICUTo monitor the radiometric performances of MAJIS using VISNIR and IR sources Specifically, there are several goals A) tracking the evolution of the actual levels (before subtracting for CDS) in the digital dynamics (0-65535 at 100 kHz, 0-4095 at 1 MHz). Such an evolution could lead to adjust an offset which can be selected by TC (4 settings) so as to avoid reaching digital saturation for the read image before analog saturation. B) tracking the evolution of the dark current and cosmetics (new hot / dead pixels) C) tracking the evolution of the overall photometric response as a function of the signal (needed for the pipeline) Pointing: MAJIS scan mirror oriented towards the ICU (8.5°) Satellite orientation: Deep space Duration: 10minMAJIS

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